The turbulent ISM and the stellar IMF

Details The turbulent ISM and the stellar IMF The turbulent ISM and the stellar IMF

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008an....329..960c&link_type=abstract

Astronomische Nachrichten, Vol.329, Issue , p.960

Astronomy and Astrophysics

Astronomy

Ism: Clouds, Ism: Kinematics And Dynamics, Ism: Structure, Stars: Formation

Scientific paper

In this contribution, we focus on the role that turbulence can play in setting the initial mass function (IMF) of stars. Two theories are contrasted. In the first, the so-called `turbulent' fragmentation theory, the turbulence is directly responsible for breaking up the cloud into `cores' which go on to form either a single star or a small N system. In such a picture, the IMF is primordial, since the mass reservoir form the young protostellar system is assumed to be set by the mass of the natal core. In the alternative picture, `competitive accretion', the final mass of a protostar is determined by its position in the potential well of the cluster. As such the IMF is determined through gravitational dynamics rather than turbulence. We discuss the observation motivation for each of these cases.

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